The posteriors for the minimum mass \(m_\mathrm {min}\)  are largely unconstrained.
As the GW detectors are less sensitive to low-mass systems, it is more difficult to place constraints on this end of the distribution [1]}, [2]}, [3]}.
The lower limit of the \(m_\mathrm {min}\)  distribution is set by our prior, and the upper limit is set by the least massive black hole amongst our observations.
